Kinematics and modeling of the inner region of M 83

Autores
Rodrigues, Irapuan; Dottori, Horacio Alberto; Diaz, Ruben Joaquin; Agüero, Maria Paz; Mast, Damian
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Two-dimensional kinematics of the central region of M 83 (NGC 5236) were obtained through three-dimensional NIR spectroscopy with the Gemini South telescope. The spatial region covered by the integral field unit (∼5″ × 13″ or ∼90 × 240 pc) was centered approximately at the center of the bulge isophotes and oriented southeast-northwest. The Paβ emission at half-arcsecond resolution clearly reveals spider-like diagrams around three centers, indicating the presence of extended masses, which we describe in terms of Satoh distributions. One of the mass concentrations is identified as the optical nucleus (ON), another as the center of the bulge isophotes, similar to the CO kinematical center (KC), and the third as a condensation hidden at optical wavelengths (hidden nucleus, HN), coincident with the largest lobe in 10 μm emission. We run numerical simulations that take into account ON, KC, and HN and four more clusters, representing the star-forming arc at the southwest of the optical nucleus. We show that ON, KC, and HN suffer strong evaporation and merge in 10-50 Myr. The star-forming arc is scattered in less than one orbital period, also falling into the center. Simulations also show that tidal striping boosts the external shell of the condensations to their escape velocity. This fact might lead to an overestimation of the mass of the condensations in kinematical observations with spatial resolution smaller than the condensations' apparent sizes. Additionally, the existence of two ILR resonances embracing the chain of H II regions, claimed by different authors, might not exist due to the similarity of the masses of the different components and the fast dynamical evolution of M 83 central 300 pc.
Fil: Rodrigues, Irapuan. Universidade Estadual da Paraiba; Brasil
Fil: Dottori, Horacio Alberto. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Diaz, Ruben Joaquin. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Agüero, Maria Paz. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Mast, Damian. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Materia
GALAXIES: INDIVIDUAL (NGC 5236)
GALAXIES: KINEMATICS AND DYNAMICS
GALAXIES: NUCLEI
GALAXIES: STELLAR CONTENT
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/214753
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/214753
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Kinematics and modeling of the inner region of M 83Rodrigues, IrapuanDottori, Horacio AlbertoDiaz, Ruben JoaquinAgüero, Maria PazMast, DamianGALAXIES: INDIVIDUAL (NGC 5236)GALAXIES: KINEMATICS AND DYNAMICSGALAXIES: NUCLEIGALAXIES: STELLAR CONTENThttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Two-dimensional kinematics of the central region of M 83 (NGC 5236) were obtained through three-dimensional NIR spectroscopy with the Gemini South telescope. The spatial region covered by the integral field unit (∼5″ × 13″ or ∼90 × 240 pc) was centered approximately at the center of the bulge isophotes and oriented southeast-northwest. The Paβ emission at half-arcsecond resolution clearly reveals spider-like diagrams around three centers, indicating the presence of extended masses, which we describe in terms of Satoh distributions. One of the mass concentrations is identified as the optical nucleus (ON), another as the center of the bulge isophotes, similar to the CO kinematical center (KC), and the third as a condensation hidden at optical wavelengths (hidden nucleus, HN), coincident with the largest lobe in 10 μm emission. We run numerical simulations that take into account ON, KC, and HN and four more clusters, representing the star-forming arc at the southwest of the optical nucleus. We show that ON, KC, and HN suffer strong evaporation and merge in 10-50 Myr. The star-forming arc is scattered in less than one orbital period, also falling into the center. Simulations also show that tidal striping boosts the external shell of the condensations to their escape velocity. This fact might lead to an overestimation of the mass of the condensations in kinematical observations with spatial resolution smaller than the condensations' apparent sizes. Additionally, the existence of two ILR resonances embracing the chain of H II regions, claimed by different authors, might not exist due to the similarity of the masses of the different components and the fast dynamical evolution of M 83 central 300 pc.Fil: Rodrigues, Irapuan. Universidade Estadual da Paraiba; BrasilFil: Dottori, Horacio Alberto. Universidade Federal do Rio Grande do Sul; BrasilFil: Diaz, Ruben Joaquin. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Agüero, Maria Paz. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Mast, Damian. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; ArgentinaIOP Publishing2009-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/214753Rodrigues, Irapuan; Dottori, Horacio Alberto; Diaz, Ruben Joaquin; Agüero, Maria Paz; Mast, Damian; Kinematics and modeling of the inner region of M 83; IOP Publishing; Astronomical Journal; 137; 5; 5-2009; 4083-40900004-62561538-3881CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/137/5/4083info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-10T13:10:32Zoai:ri.conicet.gov.ar:11336/214753instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-10 13:10:33.243CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Kinematics and modeling of the inner region of M 83
title Kinematics and modeling of the inner region of M 83
spellingShingle Kinematics and modeling of the inner region of M 83
Rodrigues, Irapuan
GALAXIES: INDIVIDUAL (NGC 5236)
GALAXIES: KINEMATICS AND DYNAMICS
GALAXIES: NUCLEI
GALAXIES: STELLAR CONTENT
title_short Kinematics and modeling of the inner region of M 83
title_full Kinematics and modeling of the inner region of M 83
title_fullStr Kinematics and modeling of the inner region of M 83
title_full_unstemmed Kinematics and modeling of the inner region of M 83
title_sort Kinematics and modeling of the inner region of M 83
dc.creator.none.fl_str_mv Rodrigues, Irapuan
Dottori, Horacio Alberto
Diaz, Ruben Joaquin
Agüero, Maria Paz
Mast, Damian
author Rodrigues, Irapuan
author_facet Rodrigues, Irapuan
Dottori, Horacio Alberto
Diaz, Ruben Joaquin
Agüero, Maria Paz
Mast, Damian
author_role author
author2 Dottori, Horacio Alberto
Diaz, Ruben Joaquin
Agüero, Maria Paz
Mast, Damian
author2_role author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: INDIVIDUAL (NGC 5236)
GALAXIES: KINEMATICS AND DYNAMICS
GALAXIES: NUCLEI
GALAXIES: STELLAR CONTENT
topic GALAXIES: INDIVIDUAL (NGC 5236)
GALAXIES: KINEMATICS AND DYNAMICS
GALAXIES: NUCLEI
GALAXIES: STELLAR CONTENT
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Two-dimensional kinematics of the central region of M 83 (NGC 5236) were obtained through three-dimensional NIR spectroscopy with the Gemini South telescope. The spatial region covered by the integral field unit (∼5″ × 13″ or ∼90 × 240 pc) was centered approximately at the center of the bulge isophotes and oriented southeast-northwest. The Paβ emission at half-arcsecond resolution clearly reveals spider-like diagrams around three centers, indicating the presence of extended masses, which we describe in terms of Satoh distributions. One of the mass concentrations is identified as the optical nucleus (ON), another as the center of the bulge isophotes, similar to the CO kinematical center (KC), and the third as a condensation hidden at optical wavelengths (hidden nucleus, HN), coincident with the largest lobe in 10 μm emission. We run numerical simulations that take into account ON, KC, and HN and four more clusters, representing the star-forming arc at the southwest of the optical nucleus. We show that ON, KC, and HN suffer strong evaporation and merge in 10-50 Myr. The star-forming arc is scattered in less than one orbital period, also falling into the center. Simulations also show that tidal striping boosts the external shell of the condensations to their escape velocity. This fact might lead to an overestimation of the mass of the condensations in kinematical observations with spatial resolution smaller than the condensations' apparent sizes. Additionally, the existence of two ILR resonances embracing the chain of H II regions, claimed by different authors, might not exist due to the similarity of the masses of the different components and the fast dynamical evolution of M 83 central 300 pc.
Fil: Rodrigues, Irapuan. Universidade Estadual da Paraiba; Brasil
Fil: Dottori, Horacio Alberto. Universidade Federal do Rio Grande do Sul; Brasil
Fil: Diaz, Ruben Joaquin. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Agüero, Maria Paz. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Mast, Damian. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
description Two-dimensional kinematics of the central region of M 83 (NGC 5236) were obtained through three-dimensional NIR spectroscopy with the Gemini South telescope. The spatial region covered by the integral field unit (∼5″ × 13″ or ∼90 × 240 pc) was centered approximately at the center of the bulge isophotes and oriented southeast-northwest. The Paβ emission at half-arcsecond resolution clearly reveals spider-like diagrams around three centers, indicating the presence of extended masses, which we describe in terms of Satoh distributions. One of the mass concentrations is identified as the optical nucleus (ON), another as the center of the bulge isophotes, similar to the CO kinematical center (KC), and the third as a condensation hidden at optical wavelengths (hidden nucleus, HN), coincident with the largest lobe in 10 μm emission. We run numerical simulations that take into account ON, KC, and HN and four more clusters, representing the star-forming arc at the southwest of the optical nucleus. We show that ON, KC, and HN suffer strong evaporation and merge in 10-50 Myr. The star-forming arc is scattered in less than one orbital period, also falling into the center. Simulations also show that tidal striping boosts the external shell of the condensations to their escape velocity. This fact might lead to an overestimation of the mass of the condensations in kinematical observations with spatial resolution smaller than the condensations' apparent sizes. Additionally, the existence of two ILR resonances embracing the chain of H II regions, claimed by different authors, might not exist due to the similarity of the masses of the different components and the fast dynamical evolution of M 83 central 300 pc.
publishDate 2009
dc.date.none.fl_str_mv 2009-05
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/214753
Rodrigues, Irapuan; Dottori, Horacio Alberto; Diaz, Ruben Joaquin; Agüero, Maria Paz; Mast, Damian; Kinematics and modeling of the inner region of M 83; IOP Publishing; Astronomical Journal; 137; 5; 5-2009; 4083-4090
0004-6256
1538-3881
CONICET Digital
CONICET
url http://hdl.handle.net/11336/214753
identifier_str_mv Rodrigues, Irapuan; Dottori, Horacio Alberto; Diaz, Ruben Joaquin; Agüero, Maria Paz; Mast, Damian; Kinematics and modeling of the inner region of M 83; IOP Publishing; Astronomical Journal; 137; 5; 5-2009; 4083-4090
0004-6256
1538-3881
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/137/5/4083
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 12.993085

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